Mass accretion to young stars triggered by flaring activity in circumstellar disks

TL;DR

This study uses 3D magnetohydrodynamic simulations to show that energetic flares in young stars can significantly perturb circumstellar disks, triggering enhanced accretion flows onto the star.

Contribution

It introduces a novel model demonstrating how stellar flares can influence disk stability and mass accretion in young star systems.

Findings

Flares create hot magnetic loops linking star and disk.

Disk material evaporates and overpressure waves propagate due to flares.

Flares can trigger funnel flows, increasing accretion onto the star.

Abstract

Young low-mass stars are characterized by ejection of collimated outflows and by circumstellar disks which they interact with through accretion of mass. The accretion builds up the star to its final mass and is also believed to power the mass outflows, which may in turn remove the excess angular momentum from the star-disk system. However, although the process of mass accretion is a critical aspect of star formation, some of its mechanisms are still to be fully understood. A point not considered to date and relevant for the accretion process is the evidence of very energetic and frequent flaring events in these stars. Flares may easily perturb the stability of the disks, thus influencing the transport of mass and angular momentum. Here we report on three-dimensional magnetohydrodynamic modeling of the evolution of a flare with an idealized non--equilibrium initial condition occurring near the disk around a rotating magnetized star. The model takes into account the stellar magnetic field, the gravitational force, the viscosity of the disk, the magnetic-field-oriented thermal conduction (including the effects of heat flux saturation), the radiative losses from optically thin plasma, and the coronal heating. We show that, during its first stage of evolution, the flare gives rise to a hot magnetic loop linking the disk to the star. The disk is strongly perturbed by the flare: disk material evaporates under the effect of the thermal conduction and an overpressure wave propagates through the disk. When the overpressure reaches the opposite side of the disk, a funnel flow starts to develop there, accreting substantial disk material onto the young star from the side of the disk opposite to the flare.